//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20140 SUBJECT: GRB 161106A: Fermi GBM detection DATE: 16/11/06 20:37:05 GMT FROM: Rachel Hamburg at UAH R. Hamburg(UAH), C. Meegan (UAH), and A von Kienlin (MPE) report on behalf of the Fermi GBM Team: "At 11:57:53.62 UT on 06 November 2016, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 161106A (trigger 500126277 / 161106499). The on-ground calculated location, using the GBM trigger data, is RA = 202.1, DEC = +64.9, with an uncertainty of 1.5 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a core-plus-tail model, with 90% of GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg systematic error [Connaughton et al. 2015, ApJS, 216, 32]. The trigger resulted in an Autonomous Repoint Request (ARR) by the GBM Flight Software owing to the high peak flux of the GRB. This ARR was accepted and the spacecraft slewed to the GBM in-flight location. The initial angle from the Fermi LAT boresight to the GBM ground location is 52 degrees. The GBM light curve consists of a single peak with a duration (T90) of about 11 s (50-300 keV). The time-averaged spectrum from T0-0.00 s to T0+16 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.61 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 125 +/- 2 keV. The event fluence (10-1000 keV) in this time interval is (1.34 +/- 0.01)E-05 (erg/cm^2). The 1-sec peak photon flux measured starting from T0+2.6 s in the 10-1000 keV band is 16.3 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20154 SUBJECT: GRB 161106A: Lomonosov BDRG gamma ray discovery DATE: 16/11/09 12:46:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs N.L.Dzhioeva,V.V.Bogomolov, S.I.Svertilov, A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, A.V.Bogomolov, A.F.Iyudin, V.V.Kalegaev, D.Nguen, V.L. Petrov, I.V.Yashin, P.S.Kazarian Physics Department, Skobel`tsyn Institute of Nuclear Physics, Lomonosov Moscow State University V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov Lomonosov Moscow State University, Sternberg Astronomical Institute I. Park, J. Lee, S. Jeong Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, Korea At 11:57:55.12 UT on 06 Nov 2016, the Lomonosov BDRG Gamma-ray Burst Monitor (http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg ), triggered GRB 161106A. GRB 161106A (R. Hamburg(UAH), GCN 20140) has one peak LC and matches with peak of Fermi Trigger event Num 495802575, total duration ~10s, the energy range 340-1100 keV. LC is available at: http://master.sai.msu.ru/static/OT/0611.jpg More information will be available at: http://lomonosov.sinp.msu.ru/category/results/observation-gamma-ray-bursts This Notice was ground-generated. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20161 SUBJECT: GRB 161106A: CALET Gamma-Ray Burst Monitor detection DATE: 16/11/09 23:58:14 GMT FROM: Takanori Sakamoto at AGU S. Nakahira (JAXA), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, Y. Yamada (AGU), K. Yamaoka (Nagoya U), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long-duration GRB 161106A (Hamburg et al., GCN Circ. 20140; Konus-Wind trigger time on 11:57:52.938) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 11:57:50.79 on 6 November 2016. The burst signal was seen by all CGBM instruments. The light curve of the SGM shows a FRED-like structure with possible overlapping pulses. The emission starts at T0, peaks at T0+5 sec and ends at T+15 sec. The T90 duration measured by the SGM data is 9.1 +- 0.5 sec (40-1000 keV). The light curve is available at http://cgbm.calet.jp/cgbm_trigger/flight/1162468560/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.